Kepler-61b is a super-Earth, an exoplanet with a radius and mass bigger than Earth, but smaller than that of the ice giants Neptune and Uranus. It has an equilibrium temperature of. It has a radius of 2.15. The mass of Kepler-61b is 6.65. At 2.15 radius and with a 6.65 mass its density would come to around 3.6 g/cm³ or slightly below the 3.9 cm³ of Mars. This planet may also have some "volatile" make up or be an ocean planet to explain the lower density.
Host star
The planet orbits a star named Kepler-61. The star has a mass of 0.63 and a radius of 0.62. It has a temperature of 4017 K and is about 1 billion years old. In comparison, the Sun is 4.6 billion years old and has a temperature of 5778 K. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 15. Therefore, it is too dim to be seen with the naked eye.
Orbit
Kepler-61b orbits its host star with about 8% of the Sun's luminosity with an orbital period of 59.877 days and an orbital radius of about 0.28 times that of Earth's. It has an eccentricity of near 0.25, meaning its orbit is mildly elliptical. It receives 27% more sunlight that Earth does.
Habitability
Kepler-61b is located in the inner part of the empirical habitable zone, a zone where liquid water could exist with high albedo, relatively low humidity and higher atmospheric pressure. However, the planet is likely tidally locked because of its close distance to its host star. It has an estimated average equilibrium temperature of, very close to that of Earth. If Kepler-61b is Earth-like it is a good candidate for life, because the system is about one billion years old, however because of its radius, it is likely gaseous, with no solid surface. However, this does not totally destroy the chances of habitability in the Kepler-61 system. Kepler-61b may well have a substantially large enough Earth-like moon, capable of supporting surface liquid water, and potentially life. However, such moons do not form naturally, it would have to be captured. For a stable orbit the ratio between the moon's orbital period Ps around its primary and that of the primary around its star Pp must be < 1/9, e.g. if a planet takes 90 days to orbit its star, the maximum stable orbit for a moon of that planet is less than 10 days. Simulations suggest that a moon with an orbital period less than about 45 to 60 days will remain safely bound to a massive giant planet or brown dwarf that orbits 1 AU from a Sun-like star. In the case of Kepler-47c, this would be practically the same to have a stable orbit. Tidal effects could also allow the moon to sustain plate tectonics, which would cause volcanic activity to regulate the moon's temperature and create a geodynamo effect which would give the satellite a strong magnetic field. However, the orbit of Kepler-61b may play a key in preventing it and the hypothetical moon from being habitable. The eccentricity of the planet is 0.25, which means it has an elliptical orbit. Kepler-61b's orbit takes it slightly beyond the inner edge of the habitable zone and then out to the middle of it, which would result in the planet experiencing temperatures of up to at is closest point in its orbit, and as low as at its farthest point. These temperatures may vary if Kepler-61b has an intense greenhouse effect, resulting in the planet being too hot to support liquid water altogether.
Discovery
In 2009, NASA's Kepler spacecraft was completing observing stars on its photometer, the instrument it uses to detect transit events, in which a planet crosses in front of and dims its host star for a brief and roughly regular period of time. In this last test, Kepler observed stars in the Kepler Input Catalog, including Kepler-61; the preliminary light curves were sent to the Kepler science team for analysis, who chose obvious planetary companions from the bunch for follow-up at observatories. The radial velocity observations confirmed that a planetary body was responsible for the dips observed in Kepler-61's light curve, thus confirming it as a planet. It was announced on April 24, 2013.
